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The high-frequency bump, characterized by a frequency exceeding ~30 Hz,represents a seldom-explored time-variability feature in the power densityspectrum (PDS) of black-hole X-ray binaries. In the 2002, 2004, 2007 and 2010outbursts of GX 339-4, the bump has been occasionally observed in conjunctionwith type-C quasi-periodic oscillations (QPOs). We systematically study theproperties of the bump during these four outbursts observed by Rossi X-rayTiming Explorer (RXTE) in the 2-60 keV bands and detect the bump in 39observations. While the frequencies of the type-C QPOs are in the range of~0.1-9 Hz, the root-mean-square (rms) amplitude of the bump shows an evolutionin the hardness ratio versus the type-C QPO frequency plot. By comparing therms amplitude of the bump with the corona temperature and simultaneous radiojet flux of the source, as previously studied in GRS 1915+105, we establishthat in the hard state of GX 339-4, the bump is always strong, with themeasurements of the rms amplitude in the range of 4-10%. At the same time, thecorona temperature is high and the radio flux is low. These findings indicatethat, using the bump as a proxy, the majority of the accretion energy isdirected towards the hot corona rather than being channeled into the radio jet.We discuss this phenomenon in terms of an inefficient energy transfer mechanismbetween the corona and jet in GX 339-4.

A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339-4